Prospects for the direct WHIM detection by Athena
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1 Exploring the Hot and Energetic Universe: 2mm The rst scientic conference dedicated to the Athena X-ray observatory Prospects for the direct WHIM detection by Athena The soft X-ray WHIM emission with WFI Andrzej M. Sołtan & Agata Różańska Nicolaus Copernicus Astronomical Center Warszawa A.M. Sołtan & Agata Różańska (NCAC) WHIM with Athena Athena Scientific Conference 1 / 27
2 Outline 1 Dark baryons 2 WHIM as seen by XMM-Newton 3 WHIM by Athena WFI A.M. Sołtan & Agata Różańska (NCAC) WHIM with Athena Athena Scientific Conference 2 / 27
3 Outline 1 Dark baryons 2 WHIM as seen by XMM-Newton 3 WHIM by Athena WFI A.M. Sołtan & Agata Różańska (NCAC) WHIM with Athena Athena Scientific Conference 3 / 27
4 A.M. Sołtan & Agata Różańska (NCAC) WHIM with Athena Athena Scientific Conference 4 / 27
5 Local baryon deficit Ω lum Ω + Ω HI + Ω X:clusters h 2 70 Ω b (0.045 ± 0.057) (Primeval abundances D, 3 He, 4 He, Li) > h 1 70 (Ly-α forest at z 2) Ω lum < Ω b < Ω m 0.3 Baryon deficyt Dark matter h 70 = H o /70 km s 1 Mpc 1 A.M. Sołtan & Agata Różańska (NCAC) WHIM with Athena Athena Scientific Conference 5 / 27
6 Four phases of baryonic matter 1 Condensed δ > 1000 T < 10 5 K stars, interstellar matter 2 Hot T > 10 7 K intracluster gas 3 Diffuse δ < 20 T < 10 5 K Ly-α forest 4 Warm 10 5 < T < 10 7 K WHIM Warm-Hot Intergalactic Medium Davé et al., ApJ, 552, 473 (2001). A.M. Sołtan & Agata Różańska (NCAC) WHIM with Athena Athena Scientific Conference 6 / 27
7 A.M. Sołtan & Agata Różańska (NCAC) WHIM with Athena Athena Scientific Conference 7 / 27 Shane & Wirtanen, Lick counts
8 Where are the baryons? A.M. Sołtan & Agata Różańska (NCAC) WHIM with Athena Athena Scientific Conference 8 / 27
9 Yoshida et al., ApJ 618, 91 (2005) A.M. Sołtan & Agata Różańska (NCAC) WHIM with Athena Athena Scientific Conference 9 / 27
10 Baryons and Dark Matter Suto et al., JKAS 37, 387 (2004) A.M. Sołtan & Agata Różańska (NCAC) WHIM with Athena Athena Scientific Conference 10 / 27
11 Outline 1 Dark baryons 2 WHIM as seen by XMM-Newton 3 WHIM by Athena WFI A.M. Sołtan & Agata Różańska (NCAC) WHIM with Athena Athena Scientific Conference 11 / 27
12 X-ray sky A.M. Sołtan & Agata Różańska (NCAC) WHIM with Athena Athena Scientific Conference 12 / 27
13 XRB vs galaxies A.M. Sołtan & Agata Różańska (NCAC) WHIM with Athena Athena Scientific Conference 13 / 27
14 XRB vs galaxies A.M. Sołtan & Agata Różańska (NCAC) WHIM with Athena Athena Scientific Conference 14 / 27
15 X-ray background (XRB) The XRB at energies above 1 kev is generated by a population of discrete extragalactic sources (mostly AGNs). At enegries below 1 kev some (basicly unknown) contribution to the XRB generate also: local (Galactic) hot plasma and the WHIM. Fluctuations of the XRB at arcmin scale are generated by a nonuniform distribution of sources contributing to the XRB: AGNs and WHIM. The WHIM is strongly correlated with galaxies. WHIM in emission: spherical halos rather than filaments. A.M. Sołtan & Agata Różańska (NCAC) WHIM with Athena Athena Scientific Conference 15 / 27
16 X-ray background (XRB) The XRB at energies above 1 kev is generated by a population of discrete extragalactic sources (mostly AGNs). At enegries below 1 kev some (basicly unknown) contribution to the XRB generate also: local (Galactic) hot plasma and the WHIM. Fluctuations of the XRB at arcmin scale are generated by a nonuniform distribution of sources contributing to the XRB: AGNs and WHIM. The WHIM is strongly correlated with galaxies. WHIM in emission: spherical halos rather than filaments. A.M. Sołtan & Agata Różańska (NCAC) WHIM with Athena Athena Scientific Conference 15 / 27
17 X-ray background (XRB) The XRB at energies above 1 kev is generated by a population of discrete extragalactic sources (mostly AGNs). At enegries below 1 kev some (basicly unknown) contribution to the XRB generate also: local (Galactic) hot plasma and the WHIM. Fluctuations of the XRB at arcmin scale are generated by a nonuniform distribution of sources contributing to the XRB: AGNs and WHIM. The WHIM is strongly correlated with galaxies. WHIM in emission: spherical halos rather than filaments. A.M. Sołtan & Agata Różańska (NCAC) WHIM with Athena Athena Scientific Conference 15 / 27
18 X-ray background (XRB) The XRB at energies above 1 kev is generated by a population of discrete extragalactic sources (mostly AGNs). At enegries below 1 kev some (basicly unknown) contribution to the XRB generate also: local (Galactic) hot plasma and the WHIM. Fluctuations of the XRB at arcmin scale are generated by a nonuniform distribution of sources contributing to the XRB: AGNs and WHIM. The WHIM is strongly correlated with galaxies. WHIM in emission: spherical halos rather than filaments. A.M. Sołtan & Agata Różańska (NCAC) WHIM with Athena Athena Scientific Conference 15 / 27
19 X-ray background (XRB) The XRB at energies above 1 kev is generated by a population of discrete extragalactic sources (mostly AGNs). At enegries below 1 kev some (basicly unknown) contribution to the XRB generate also: local (Galactic) hot plasma and the WHIM. Fluctuations of the XRB at arcmin scale are generated by a nonuniform distribution of sources contributing to the XRB: AGNs and WHIM. The WHIM is strongly correlated with galaxies. WHIM in emission: spherical halos rather than filaments. A.M. Sołtan & Agata Różańska (NCAC) WHIM with Athena Athena Scientific Conference 15 / 27
20 Whim emission expected extremely weak stacking of observations Azimuthal symmentry X-ray sky cross-correlation function XMM-Newton archive Galaxy data APM + MAPS catalogue (17 20 mag, 0.06 z 0.22) 150 pointings s 20 galaxies s Order of magnitude deeper than 4Ms CDFS A.M. Sołtan & Agata Różańska (NCAC) WHIM with Athena Athena Scientific Conference 16 / 27
21 Whim emission expected extremely weak stacking of observations Azimuthal symmentry X-ray sky cross-correlation function XMM-Newton archive Galaxy data APM + MAPS catalogue (17 20 mag, 0.06 z 0.22) 150 pointings s 20 galaxies s Order of magnitude deeper than 4Ms CDFS A.M. Sołtan & Agata Różańska (NCAC) WHIM with Athena Athena Scientific Conference 16 / 27
22 Whim emission expected extremely weak stacking of observations Azimuthal symmentry X-ray sky cross-correlation function XMM-Newton archive Galaxy data APM + MAPS catalogue (17 20 mag, 0.06 z 0.22) 150 pointings s 20 galaxies s Order of magnitude deeper than 4Ms CDFS A.M. Sołtan & Agata Różańska (NCAC) WHIM with Athena Athena Scientific Conference 16 / 27
23 Whim emission expected extremely weak stacking of observations Azimuthal symmentry X-ray sky cross-correlation function XMM-Newton archive Galaxy data APM + MAPS catalogue (17 20 mag, 0.06 z 0.22) 150 pointings s 20 galaxies s Order of magnitude deeper than 4Ms CDFS A.M. Sołtan & Agata Różańska (NCAC) WHIM with Athena Athena Scientific Conference 16 / 27
24 Whim emission expected extremely weak stacking of observations Azimuthal symmentry X-ray sky cross-correlation function XMM-Newton archive Galaxy data APM + MAPS catalogue (17 20 mag, 0.06 z 0.22) 150 pointings s 20 galaxies s Order of magnitude deeper than 4Ms CDFS A.M. Sołtan & Agata Różańska (NCAC) WHIM with Athena Athena Scientific Conference 16 / 27
25 Whim emission expected extremely weak stacking of observations Azimuthal symmentry X-ray sky cross-correlation function XMM-Newton archive Galaxy data APM + MAPS catalogue (17 20 mag, 0.06 z 0.22) 150 pointings s 20 galaxies s Order of magnitude deeper than 4Ms CDFS A.M. Sołtan & Agata Różańska (NCAC) WHIM with Athena Athena Scientific Conference 16 / 27
26 Whim emission expected extremely weak stacking of observations Azimuthal symmentry X-ray sky cross-correlation function XMM-Newton archive Galaxy data APM + MAPS catalogue (17 20 mag, 0.06 z 0.22) 150 pointings s 20 galaxies s Order of magnitude deeper than 4Ms CDFS A.M. Sołtan & Agata Różańska (NCAC) WHIM with Athena Athena Scientific Conference 16 / 27
27 Whim emission expected extremely weak stacking of observations Azimuthal symmentry X-ray sky cross-correlation function XMM-Newton archive Galaxy data APM + MAPS catalogue (17 20 mag, 0.06 z 0.22) 150 pointings s 20 galaxies s Order of magnitude deeper than 4Ms CDFS A.M. Sołtan & Agata Różańska (NCAC) WHIM with Athena Athena Scientific Conference 16 / 27
28 Whim emission expected extremely weak stacking of observations Azimuthal symmentry X-ray sky cross-correlation function XMM-Newton archive Galaxy data APM + MAPS catalogue (17 20 mag, 0.06 z 0.22) 150 pointings s 20 galaxies s Order of magnitude deeper than 4Ms CDFS A.M. Sołtan & Agata Różańska (NCAC) WHIM with Athena Athena Scientific Conference 16 / 27
29 Correlation analysis The WHIM is strongly correlated with the galaxy distribution. At small angular scales, the WHIM structure defines the signal of the cross-correlation function (CCF). At large scales the CCF signal is generated by the large scale fluctuations of the galaxy distribution (the galaxy autocorrelation function). δρ(θ) = s P(θ) + s w gg (θ) n g δρ(θ) average excess of the X-ray flux, s brightness of the individual WHIM halo around galaxy, P(θ) normalized surface brightness of the WHIM halo, w gg (θ) autocorrelation function of galaxies, n g surface density of galaxies surrounded by the WHIM halos. A.M. Sołtan & Agata Różańska (NCAC) WHIM with Athena Athena Scientific Conference 17 / 27
30 Correlation analysis The WHIM is strongly correlated with the galaxy distribution. At small angular scales, the WHIM structure defines the signal of the cross-correlation function (CCF). At large scales the CCF signal is generated by the large scale fluctuations of the galaxy distribution (the galaxy autocorrelation function). δρ(θ) = s P(θ) + s w gg (θ) n g δρ(θ) average excess of the X-ray flux, s brightness of the individual WHIM halo around galaxy, P(θ) normalized surface brightness of the WHIM halo, w gg (θ) autocorrelation function of galaxies, n g surface density of galaxies surrounded by the WHIM halos. A.M. Sołtan & Agata Różańska (NCAC) WHIM with Athena Athena Scientific Conference 17 / 27
31 Correlation analysis The WHIM is strongly correlated with the galaxy distribution. At small angular scales, the WHIM structure defines the signal of the cross-correlation function (CCF). At large scales the CCF signal is generated by the large scale fluctuations of the galaxy distribution (the galaxy autocorrelation function). δρ(θ) = s P(θ) + s w gg (θ) n g δρ(θ) average excess of the X-ray flux, s brightness of the individual WHIM halo around galaxy, P(θ) normalized surface brightness of the WHIM halo, w gg (θ) autocorrelation function of galaxies, n g surface density of galaxies surrounded by the WHIM halos. A.M. Sołtan & Agata Różańska (NCAC) WHIM with Athena Athena Scientific Conference 17 / 27
32 Correlation analysis The WHIM is strongly correlated with the galaxy distribution. At small angular scales, the WHIM structure defines the signal of the cross-correlation function (CCF). At large scales the CCF signal is generated by the large scale fluctuations of the galaxy distribution (the galaxy autocorrelation function). δρ(θ) = s P(θ) + s w gg (θ) n g δρ(θ) average excess of the X-ray flux, s brightness of the individual WHIM halo around galaxy, P(θ) normalized surface brightness of the WHIM halo, w gg (θ) autocorrelation function of galaxies, n g surface density of galaxies surrounded by the WHIM halos. A.M. Sołtan & Agata Różańska (NCAC) WHIM with Athena Athena Scientific Conference 17 / 27
33 CCF at high energies Sołtan, A&A 460, 59 (2006) A.M. Sołtan & Agata Różańska (NCAC) WHIM with Athena Athena Scientific Conference 18 / 27
34 CCF at soft energies Sołtan, A&A 460, 59 (2006) A.M. Sołtan & Agata Różańska (NCAC) WHIM with Athena Athena Scientific Conference 19 / 27
35 WHIM surface brightness profile Sołtan, A&A 460, 59 (2006) A.M. Sołtan & Agata Różańska (NCAC) WHIM with Athena Athena Scientific Conference 20 / 27
36 Outline 1 Dark baryons 2 WHIM as seen by XMM-Newton 3 WHIM by Athena WFI A.M. Sołtan & Agata Różańska (NCAC) WHIM with Athena Athena Scientific Conference 21 / 27
37 E = KeV σ = (2 3) 10 8 cnt s 1 pxl 1 σ = cnt s 1 arcmin 1 1 cnt = erg cm 2 σ = ph cm 2 s 1 arcmin 1 A.M. Sołtan & Agata Różańska (NCAC) WHIM with Athena Athena Scientific Conference 22 / 27
38 WFI ARF (no filter) A.M. Sołtan & Agata Różańska (NCAC) WHIM with Athena Athena Scientific Conference 23 / 27
39 WFI background A.M. Sołtan & Agata Różańska (NCAC) WHIM with Athena Athena Scientific Conference 24 / 27
40 Signal against Noise n = ARF σ S = n A t exp N = b A t exp S/N = n A texp b where: n count excess generated by WHIM per arcmin 2 A solid angle of the WHIM halo t exp exposure time A.M. Sołtan & Agata Różańska (NCAC) WHIM with Athena Athena Scientific Conference 25 / 27
41 S/N for two mirror modules on-axis A.M. Sołtan & Agata Różańska (NCAC) WHIM with Athena Athena Scientific Conference 26 / 27
42 Athena most likely will have the capability to detect the soft X-ray emission from individual WHIM halos accumulated around nearby galaxies. A moderate exposure time would be required. Imaging of the detailed structure will need long but still feasible exposures. Thank you A.M. Sołtan & Agata Różańska (NCAC) WHIM with Athena Athena Scientific Conference 27 / 27
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